Event Detail Information
Spherical polar coordinates have many desirable properties for simulations in relativistic astrophysics. In the absence of symmetry conditions, however, numerical relativity simulations in spherical polar coordinates have been hampered by problems associated with coordinate singularities. In this talk I will discuss a new approach that does not require regularization of the singular terms, and instead employs a reference-metric formulation of the BSSN equations, a proper rescaling of the dynamical variables, and a partially-implicit Runge-Kutta integration scheme. I will review these ingredients, and will then present some tests and early applications.